Sample records for zemtsovsky galina zemtsovskaya
-
Watt, Timothy J; Duan, Jian J
2014-08-01
Spathius galinae Belokobylskij and Strazenac (Hymenoptera: Braconidae) is a recently discovered gregarious idiobiont larval ectoparasitoid currently being evaluated for biological control against the invasive emerald ash borer, Agrilus planipennis Fairmaire (Coleoptera: Buprestidae) in the United States. To aid in the development of laboratory rearing protocols, we assessed the influence of various emerald ash borer stages on critical fitness parameters of S. galinae. We exposed gravid S. galinae females to emerald ash borer host larvae of various ages (3.5, 5, 7, and 10 wk post egg oviposition) that were reared naturally in tropical (evergreen) ash (Fraxinus uhdei (Wenzig) Lingelsh) logs, or to field-collected, late-stage emerald ash borers (nonfeeding J-shaped larvae termed "J-larvae," prepupae, and pupae) that were artificially inserted into green ash logs. When exposed to larvae in tropical ash logs, S. galinae attacked 5 and 7 wk hosts more frequently (68-76%) than 3.5 wk (23%) and 10 wk (12%) hosts. Subsample dissections of the these logs revealed that 3.5, 5, 7 and 10 wk host logs contained mostly second, third, fourth, and J-larvae, respectively, that had already bored into the sapwood for diapause. No J-larvae were attacked by S. galinae when naturally reared in tropical ash logs. When parasitized by S. galinae, 7 and 10 wk hosts produced the largest broods (approximately 6.7 offspring per parasitized host), and the progenies that emerged from these logs had larger anatomical measurements and more female-biased sex ratios. When exposed to emerald ash borer J-larvae, prepupae, or pupae artificially inserted into green ash logs, S. galinae attacked 53% ofJ-larvae, but did not attack any prepupae or pupae. We conclude that large (fourth instar) emerald ash borer larvae should be used to rear S. galinae.
-
Duan, Jian J; Watt, Timothy J; Larson, Kristi
2014-06-01
Spathius galinae Belokobylskij & Strazanac is a recently described parasitoid of the emerald ash borer, Agrilus planipennis Fairmaire, in the Russian Far East, and is currently being considered for biocontrol introduction in the United States. Using A. planipennis larvae reared with freshly cut ash (Fraxinus spp.) sticks, we investigated the biology, life cycle, and rearing of S. galinae in the laboratory under normal rearing conditions (25 +/- 1 degrees C, 65 +/- 10% relative humidity, and a photoperiod of 16:8 [L:D] h). Our study showed that S. galinae took approximately 1 mo (29 d) to complete a single generation (from egg to adult) under the laboratory rearing conditions. After eclosion from eggs, larvae of S. galinae molted four times to reach the fifth instar, which then spun cocoons for pupation and development to adults. Adult female wasps had a median survival time of 7 wk with fecundity peaking 3 wk after emergence when reared in groups (of five females and five males) and 2 wk in single pairs. Throughout the life span, a single female S. galinae produced a mean (+/- SE) of 31 (+/- 3.0) progeny when reared in groups, and a mean (+/- SE) of 47 (+/- 5.3) progeny when reared in single pairs. Results from our study also showed that S. galinae could be effectively reared with A. planipennis larvae reared in both green (Fraxinus pennsylvanica Marshall) and tropical [Fraxinus uhdei (Wenzig) Lingelsh] ash sticks. However, the abortion (unemergence) rate of S. galinae progeny was much higher (20%) when reared with host larvae in green ash sticks than that (2.1%) in tropical ash sticks.
-
USDA-ARS?s Scientific Manuscript database
Emerald ash borer Agrilus planipennis Fairmaire (Coleoptera: Buprestidae) is an invasive pest of serious concern in North America. To complement ongoing biological control efforts, Spathius galinae Belokobylskij and Strazenac (Hymenoptera: Braconidae), a recently-described specialist parasitoid of ...
-
USDA-ARS?s Scientific Manuscript database
Spathius galinae Belokobylskij and Strazenac (Hymenoptera: Braconidae) is a recently discovered gregarious idiobiont larval ectoparasitoid currently being evaluated for biological control against the invasive emerald ash borer, Agrilus planipennis Fairmaire (Coleoptera: Buprestidae) in the United St...
-
USDA-ARS?s Scientific Manuscript database
Spathius galinae Belokobylskij & Strazajac is a recently described parasitoid of the emerald ash borer, Agrilus plannipennis Fairmaire, in the Russian Far East, and is currently being considered for biocontrol introduction in the US. Using A. planipennis larvae reared with freshly cut ash (Fraxinus ...
-
USDA-ARS?s Scientific Manuscript database
Producing insect natural enemies in laboratories or insectaries for biological pest control is often expensive, and developing cost-effective rearing techniques is a goal of many biological control programs. Spathius galinae Belokobylskij and Strazenac (Hymenoptera: Braconidae), a recently described...
-
EPR of Nd3+ in congruent and nearly stoichiometric lithium niobate
NASA Astrophysics Data System (ADS)
Malovichko, G.; Grachev, V.; Okulov, S.; Kokanyan, E.; Henecker, F.; Hofstaetter, A.; Schirmer, O.
2006-02-01
The cover picture refers to the article by Galina Malovichko et al. which has been selected as Editor's Choice for this issue [1]. The lower part of the figure shows a section of the angular dependence of the EPR spectra in the xy-plane for nearly stoichiometric LiNbO3:Nd3+. The solid lines correspond to non-magnetic neodymium isotopes of axial C3 symmetry (green) and low C1 symmetry (purple and blue), respectively; the symbols represent experimental data. The upper part of the figure shows possible structures of the nearest surrounding for the C3 and C1 centers and their correspondence to the observed line positions.The first author Galina Malovichko is Associate Professor in the Physics Department at the Montana State University, USA. Her scientific activity is devoted to experimental condensed matter physics, particularly to the study of structures of extrinsic, intrinsic and radiation defects and their influence on crystal prop-erties. Her group is involved in the characterization of various materials and optimization of their parameters for advanced ap-plications.
-
USDA-ARS?s Scientific Manuscript database
Host-specificity determination prior to the introduction of non-native natural enemies (predators and parasitoids) is a critical component of the risk assessment for modern classical biological control programs. In the present study, we assessed the host specificity of a newly described parasitoid,...
-
JPRS Report, Soviet Union, Political Affairs
1989-09-27
the popular "On-Duty Reporter" column , Yeliza- veta Bogoslovskaya, Sergey Chesnokov, and Galina Sapunova, literally have not gotten off the telephone...Affairs E . A. Didorenko. He has demonstrated the kind of admirable energy that he has failed to show in the fight against crime. Back on 23 February...Our editorial welcomed E . A. Didorenko’s and TASH- KENTSKAYA PRAVDA’s desire to shed light on many problems of interethnic relations and the
-
2016-10-27
Institute of Infectious Diseases, Fort Detrick, Frederick, Maryland, USA 9 10 11 Running head: Complete Genome Sequence of Y. pestis strain Cadman...1 Complete Genome Sequence of Pigmentation Negative Yersinia pestis strain Cadman 1 2 3 Sean Lovetta, Kitty Chaseb, Galina Korolevaa, Gustavo...we report the genome sequence of Yersinia pestis strain Cadman, an attenuated strain 25 lacking the pgm locus. Y. pestis is the causative agent of
-
Zhang, Jian-Min; Shen, Hai-Yan; Liao, Ming; Ren, Tao; Guo, Li-Li; Xu, Cheng-Gang; Feng, Sai-Xiang; Fan, Hui-Ying; Li, Jing-Yi; Chen, Ji-Dang; Zhang, Bin
2012-04-24
Haemophilus parasuis is the etiological agent of Glässer's disease, which is characterised by fibrinous polyserositis, meningitis and polyarthritis, causing severe economic losses to the swine industry. In this study, a loop-mediated isothermal amplification (LAMP) test was developed to improve the specificity, facility and speed of diagnosis of H. parasuis isolates. The LAMP assay rapidly amplified the target gene within 50 min incubation at 63 °C in a laboratory water bath. The LAMP amplicon could be visualised directly in the reaction tubes following the addition of SYBR Green I dye. The detection limit of this LAMP method was 10 CFU/mL, which was 10 times more sensitive than the earlier 16S rRNA polymerase chain reaction (PCR) test conducted by Oliveira, Galina and Pijoan (2001), and no cross-reactivity was observed from other non-H. parasuis strains. This LAMP test was evaluated further on 187 clinical specimens from pigs suspected of being infected with H. parasuis. Forty-three were found positive by bacterial isolation of H. parasuis, as well as by the 16S rRNA PCR and LAMP tests. The 43 H. parasuis isolates were classified into 9 serovars and had 37 genetic patterns when analysed by pulsed-field gel electrophoresis (PFGE). This displayed that various H. parasuis serovars and genotypes were widely distributed in South China. Therefore, the speed, specificity and sensitivity of the LAMP test, the lack of a need for expensive equipment, and the visual readout showed great potential for a correct clinical diagnosis of H. parasuis in favour of controlling Glässer's disease.
-
NASA Astrophysics Data System (ADS)
Kuznetsov, E.; Kaiser, G.
2003-04-01
The paper is concerned with the determination of the second sectorial harmonic parameters of geopotential using the positional observations of the geosynchronous satellites at the Kourovka Astronomical Observatory. The calculated corrections Delta C_{22} and Delta S_{22} for the geopotential model JGM-3 are equal to Delta C_{22}=(-2.6 ± 1.4) * 10(-10) , Delta S_{22}=(-3.1 ± 0.9) * 10(-10) . From ads Wed Jan 12 06:25:03 2005 Return-Path:
Received: (from ads@localhost) by head.cfa.harvard.edu (d/w) id j0CBP3DC007102; Wed, 12 Jan 2005 06:25:03 -0500 (EST) Received: from cfa.harvard.edu (cfa.harvard.edu [131.142.10.1]) by head.cfa.harvard.edu (d/w) with ESMTP id j0CBOeKD007030 for -
Decontamination of radionuclides using γ-Fe2O3 as a Nanosorbent
NASA Astrophysics Data System (ADS)
Bagla, Hemlata; Thakur, Jyotsna
2017-04-01
The release of radioactive waste into the environment and the disposal of conditioned waste is a major environmental concern which demands the improvement in the remediation processes [1]. Due to the advancements in Nanotechnology, novel and simple nanoparticles have been proved very efficient worldwide, in the radioactive waste treatment processes [2]. These nanoparticles prove to be an excellent nanosorbents owing to its very high surface area and other size dependent properties [3]. In the present study, nanocrystalline γ-Fe2O3 was synthesized by gel-combustion method. Gel combustion method [4, 5] is the most facile method of synthesis of nanocrystalline oxides. Fuel deficient composition of ferric nitrate (oxidant) and malonyl dihydrazide (fuel) were mixed well in de-ionised water and heated at temperature 300 °C. The smouldering combustion took place resulting in formation of γ-Fe2O3 which further calcined at 500 °C to remove undesirable impurities. The prepared powder further characterized by various techniques such as X-ray diffractometer, transmission electron microscopy, BET technique and zeta potential measurements. The crystallite size of γ-Fe2O3 was found to be 11 nm. TEM images showed that the grain size obtained was in agreement with the XRD report. Sorption study have been carried out using tracer technique for batch equilibration method at room temperature and atmospheric pressure. A known amount of sorbent (γ-Fe2O3) was mixed with 10 mL of solution containing radiotracer and 1mg/mL solution of carrier. Various parameters such as contact time, pH, amount of sorbent, concentration, temperature, agitation speed were optimized, determination of sorption capacity and interference study was also conducted. The activity is measured by using single channel NaI(Tl) well type gamma ray spectrometer. γ-Fe2O3 was found to be an efficient and cost effective sorbent for the decontamination of heavy radionuclides such as Cs-137, Sr-90, Cd-115m, Cr-51, Hg-203, etc. from low level waste and water effluent. References: 1. Hamasaki T., Nakamichi N., Teruya K., Shirahata S., Removal Efficiency of Radioactive Cesium and Iodine Ions by a Flow-Type Apparatus Designed for Electrochemically Reduced Water Production, PLoS One. 2014; 9(7): e102218. 2. Gehrke I., Geiser A., Somborn-Schulz A., Innovations in nanotechnology for water treatment, Nanotechnol Sci Appl. 2015; 8: 1-17. 3. Galina Lujanienė G., Šemčuk S., Kulakauskaitė I., Mažeika K., Valiulis D., Ju\\vskėnas R., Tautkus S., Sorption of radionuclides and metals to graphene oxide and magnetic graphene oxide, Journal of Radioanalytical and Nuclear Chemistry, 2016;307:3, 2267-2275 4. Patil K.C., Hegde M.S., Rattan T., Aruna S.T., Chemistry of Nanocrystalline Oxide Materials Combustion Synthesis, Properties and Applications, world Scientific Publ. 2008. 5. Thakur, J., Dutta, D. P., Bagla, H. and Tyagi, A. K., Effect of Host Structure and Concentration on the Luminescence of Eu3+ and Tb3+ in Borate Phosphors., J. Am. Ceram. Soc., 2012, 95: 696-704.
-
NASA Astrophysics Data System (ADS)
Yushchenko, A.; Kim, C.; Sergeev, A.
2003-04-01
Quasar-galaxy associations can be explained as gravitational lensing by globular clusters, located in the halos of the foreground galaxies and dwarf galaxies in small groups of galaxies. We propose an observational test for checking this hypothesis. We used the SUPERCOSMOS sky survey to find the overdensities of star-like sources with zero proper motions in the vicinities of the~foreground galaxies from the CfA3 catalog. The results obtained for 19413 galaxies are presented. We show the results of calculations of number densities of star-like sources with zero proper motions in the vicinity of 19413 galaxies. Two different effects can explain the observational data: lensing by globular clusters and lensing by dwarf galaxies. We carried out the CCD 3-color photometry with the 2.0-m telescope of the~Terskol Observatory and the 1.8-m telescope of the Bohyunsan Observatory (South Korea) to select extremely lensed objects around several galaxies for future spectroscopic observations. From ads Wed Jan 12 06:25:17 2005 Return-Path:
Received: (from ads@localhost) by head.cfa.harvard.edu (d/w) id j0CBPHjt007159; Wed, 12 Jan 2005 06:25:17 -0500 (EST) Received: from cfa.harvard.edu (cfa.harvard.edu [131.142.10.1]) by head.cfa.harvard.edu (d/w) with ESMTP id j0CBOuKD007095 for -
Shoemaker-Levy 9/JUPITER Collision Update
NASA Astrophysics Data System (ADS)
1994-05-01
There are many signs that the upcoming collision between comet Shoemaker-Levy 9 and giant planet Jupiter is beginning to catch the imagination of the public. Numerous reports in the various media describe the effects expected during this unique event which according to the latest calculations will start in the evening of July 16 and end in the morning of July 22, 1994. (The times in this Press Release are given in Central European Summer Time (CEST), i.e., Universal Time (UT) + 2 hours. The corresponding local time in Chile is CEST - 6 hours.) Astronomers all over the world are now preparing to observe the associated phenomena with virtually all major telescopes. There will be no less than 12 different investigations at the ESO La Silla observatory during this period. This Press Release updates the information published in ESO PR 02/94 (27 January 1994) and provides details about the special services which will be provided by ESO to the media around this rare astronomical event. SCIENTIFIC EXPECTATIONS The nucleus of comet Shoemaker-Levy 9 broke into many smaller pieces during a near passage of Jupiter in July 1992. They are now moving in parallel orbits around this planet and recent calculations show with close to 100 % certainty that they will all collide with it, just two months from now. At some time, more than 20 individual nuclei were observed. This Press Release is accompanied by a photo that shows this formation, the famous "string of pearls", as it looked like in early May 1994. Both Jupiter and these nuclei have been extensively observed during the past months. A large, coordinated observing programme at La Silla has been active since early April and the first results have become available. However, while we now possess more accurate information about the comet's motion and the times of impact, there is still great uncertainty about the effects which may actually be observed at the time of the impacts. This is first of all due to the fact that it has not been possible to measure the sizes and masses of the individual cometary nuclei and thereby to estimate the amount of energy which will be liberated at the collisions. The first object (nucleus "A"; indicated on the photo) will hit the Jovian atmosphere somewhat later than earlier predicted; the best estimate is now at about 22:00 CEST in the evening of Saturday, 16 July, 1994. The second ("B") will follow the next morning at about 05:00. These two nuclei are comparatively faint and therefore presumably also rather small, and it is at this moment still uncertain whether these impacts will actually be observed. The first, relatively large nuclei ("E") will hit Jupiter around 17:00 on 17 July. The brightest nucleus ("Q"; actually a double object, as seen on images obtained with the Hubble Space Telescope) is expected to arrive just before 22:00 on 20 July, and the last in the train ("W") should collide with the planet at about 10:20 on 22 July. The timing uncertainty varies from impact to impact; in the best cases, there is at present a 95% chance that the collision will happen between 40 minutes before and 40 minutes after the indicated time. Further positional observations are being obtained, also at ESO, and it is hoped that this margin can be reduced to about +-15 minutes or better. Despite intensive spectroscopic observations, no gas has yet been detected in any of the nuclei. We only see dust around the nuclei which are completely hidden from our view within these clouds. The amount of the dust has been steadily decreasing; this is because the dust production from the individual nuclei -- which began when the parent body broke up at the time of the near-collision with Jupiter in July 1992 -- is slowly diminishing with time. Some of the smaller nuclei have recently disappeared from view, probably because they have ceased to produce dust. It is not clear, however, whether this also implies that they no longer exist at all, or whether they are just too small to be seen with available telescopes. THE ESO COORDINATED PROGRAMME Together with their colleagues all over the world, several groups of astronomers in the ESO member states are now getting ready to observe this event with the La Silla telescopes. The observers at ESO participate in a coordinated programme and will profit from the simultaneous observations with many different telescopes and observing techniques at one site. Altogether, there are 12 individual programmes at all the major telescopes, including the 3.6-m, the NTT, the SEST, the 2.2-m MPI/ESO, the 1.4-m CAT and the Danish 1.54-m telescopes. It is clear that these observations will be difficult, in particular because of the relatively short time that Jupiter and the comet will be well above the horizon at La Silla, at most a few hours each evening. When Jupiter is very low in the sky, the viewing conditions are less favourable, since the light must traverse a longer distance through the turbulent and absorbing terrestrial atmosphere. However, since Jupiter will be south of the celestial equator, observing conditions will be even worse from observatories located in the Northern hemisphere. To record the best possible data (images, spectra, light curves, etc.), the telescopes must follow the motion of Jupiter very accurately. Due to its orbital motion in the solar system, Jupiter moves rather rapidly in the sky, and the telescope motion must be precisely offset to continuously track the planet without "smearing" the images. This is not a simple task, also since the planet's rate of motion changes with time and new corrections must be made several times each hour. All in all, the observers face a difficult task and must be extremely alert, especially around the predicted moments of impact. This will demand very high concentration and necessitate "training runs" before the real observations begin. Some of these have already taken place -- not surprisingly, various technical problems were uncovered and are now in the process of being resolved. ESO'S SERVICES TO THE MEDIA In view of the unique nature of this event and the associated astronomical observations, ESO has decided to provide special services to the media. In particular, it is the intention to ensure that the media will be able to follow the developments at La Silla closely and in near-real time, and at the same time will be kept informed about the observational results at other observatories all over the world. This service will be available from the ESO Headquarters in Garching near Munich, Germany, but special arrangements will also be made for the media in Chile. Kindly note that in view of the complex and critical nature of these observations, it is not possible to arrange direct access to the La Silla observatory during the observing period. ESO will obtain all new information directly from the observers at La Silla via the permanent satellite link to the ESO Headquarters in Garching (Germany). For this, ESO is setting up the necessary internal communication lines at La Silla which will allow this transfer to be done at the shortest possible notice. While the observers cannot be disturbed during the actual observations, they will communicate their results and observational progress at regular intervals, and very quickly, if and when "dramatic" events are observed. ESO furthermore has complete and permanent access to the world-wide communication net between all observers of this event, especially set up for this purpose. The information available from this source will first of all serve to alert the observers about the results in other places and to warn them about new and unexpected developments. Moreover, the Space Telescope European Coordinating Facility, the ESA/ESO group that is responsible for the Hubble Space Telescope use by European astronomers and which is housed at the ESO Headquarters, will contribute with information regarding the observations with this major observational facility. With these important sources of information at its disposal, ESO will therefore be in a prime position to inform about and comment on the latest developments at the shortest possible notice. SPECIFIC ARRANGEMENTS In practical terms, ESO's service to the media will have the following elements: - Background material in the form of text and images, as well as related video clippings (broadcast quality) will be available at request, 7 - 10 days before the first impact takes place on 16 July. - Beginning a few days before this date, ESO will issue daily bulletins with the latest predictions and other news, related to the preparations of observations at La Silla and elsewhere in the world. - ESO will arrange a Press Conference at the ESO Headquarters in Garching at 20:00 (CEST) on Saturday 16 July, 1994. This will be just before the first impact is expected to happen and will provide an excellent opportunity to inform the media about the very latest developments. Following this in-depth briefing, media representatives are welcome to pass the night at the ESO Headquarters and to follow the first observations at La Silla at distance (food and beverages will be provided). Unexpected and "spectacular" events, should they happen, will be announced and commented as quickly as possible. We will also attempt to contact the La Silla observers by phone immediately after the end of their observations (in the early morning hours at Garching) and request live commentaries about the intial results. At the same time, the latest images will be transferred and made available. - There will be a Press Conference each day at 11:00 (CEST) on 17 - 22 July 1994, summarizing the previous night's results. Selected images obtained at ESO the night before will be available on these occasion. Media representatives, who are interested in participating in the Press Conference in the evening of July 16 and who would like to stay at ESO during the following night, are kindly requested to soonest contact Mrs. E. Voelk of the ESO Information Service (Tel.: +4989-32006276; Fax: +4989-3202362), to obtain a personal invitation. ESO is preparing special arrangements for the Chilean media; they will soon be announced directly to the involved. PHOTO CAPTION ESO PR PHOTO 10/94-1: PORTRAIT OF A DOOMED COMET These two photos from the ESO La Silla observatory show the individual nuclei of comet Shoemaker-Levy 9, now headed for collision with Jupiter on 16 - 22 July 1994. The wide-field photo (below, left) was obtained by Klaus Jockers and Galina Chernova (Max-Planck-Institute fur Aeronomie, Katlenburg, Lindau, Germany) on May 1, 1994. For this 5 min exposure in red light they used a CCD camera at the MPIfAe/Hoher List focal reducer at the ESO 1-metre telescope. The entire nuclear train (the "string of pearls") is very well seen, together with the sunlight-reflecting dust from the nuclei, all on one side. On this date, the comet was 654 million km from the Earth and the angular extension of the train was about 5.3 arcmin, corresponding to a projected length of just over 1 million km. A 15 min CCD image was obtained for astrometric purposes on May 11, 1994, by Jean-Francois Claeskens at the Danish 1.5 m telescope at La Silla; it is here reproduced in close-up to show well the individual nuclei, in particular the fainter ones. The bright object to the upper right is a 10th mag star. Note that the stars in the field are somewhat trailed, since the telescope was set to follow the motion of the comet. The first nucleus to hit Jupiter will be "A", here seen 42 mm from the left edge and 33 mm below the upper edge of the large picture. The last is "W", 43 mm above the lower edge and 9 mm from the right edge. The comet was 657 million km from the Earth and the train was somewhat longer, 5.8 arcmin, i.e. the projected length was now 1.1 million km. Technical information: Wide-Field: pixel size 1.5 arcsec; scale on photo: 5.1 arcsec/mm; field size: 12.2 x 6.6 arcmin; 5 min exposure; gunn-r filtre. Close-Up: pixel size 0.38 arcsec; scale on photo: 1.3 arcsec/mm; field size: 6.4 x 4.4 arcmin; 15 min exposure; V-filtre. On both photos, North is up and East is to the left; both were obtained during moderate seeing conditions.